J/A+A/691/A249ivo://CDS.VizieR/J/A+A/691/A249doi:10.26093/cds/vizier.36910249CDSSaez-Carvajal C.Vogt N.Zorotovic M.Garcia-Veas J.Aravena-Rojas G.,Dumond L.Figueroa-Tapia F.Lopez-Bonilla Y.Rodriguez-Jimenez A.,Vega-Manubens I.Grawe B.2025-03-19T20:02:21Z2024-11-19T13:01:05ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frvariable-starscataclysmic-variable-starseclipsing-binary-starsThe orbital period of a cataclysmic variable stands as a crucial parameter for investigating the structure and physics of these binary systems, as well as understanding their evolution. We use photometric Gaia data of dwarf novae (DNe) in the quiescent state, available over various years, to determine new orbital periods and improve or modify previously suggested period values. Two approaches are implemented for selecting high-inclination targets, either eclipsing or with ellipsoidal variations. We determine new orbital periods for 75 DNe and improve ephemerides for 27 more (three of which change significantly), contributing to 9.4% of the known DNe periods between 0.05 and 2.0 days, and doubling those with periods exceeding 0.44 days. Their phase-folded light curves, available on Zenodo, are presented and arranged by their orbital period, illustrating the transition from short-period systems, dominated by radiation from the accretion disk and the hot spot, to longer-period DNe, where the Roche-lobe filling secondary star is the primary visual flux source. This transition, which occurs around the well-known period gap (between ~ 2 and 3 hours), is expected since DNe with larger orbital periods typically harbour more massive donors contributing to the visible flux. However, this transition is not abrupt. Within the same range of periods, we observe systems dominated by ellipsoidal variations, where the companion star is clearly visible, as well as others dominated by the disk and the hot spot. The presence of some DNe with ellipsoidal variations near the lower edge of the period gap is striking, as the companions in these systems are expected to be cool low-mass M-dwarfs not visible in the light curve. This could indicate that we are observing systems where the donor star was originally much more massive and underwent significant nuclear evolution before mass transfer began, as has been suggested previously for QZ Ser.2024A&A...691A.249Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/691/A249CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/691/A249https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/691/A249http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/691/A249https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/691/A249https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/691/A249http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/691/A249GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/691/A249/sources (List of studied sources)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/691/A249/sources?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/691/A249/sources?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/691/A249/sources?GETtext/xml+votable180.050000true0.59333342.7036110.0055555555555555566/1141 2405 2461 2506 2659 2731 2956 2981 3039 3225 3236 3287 3509 5457 6925 7981 10242 12471 12792 12798 13023 13054 13249 13307 13832 13896 14065 14446 14596 14642 14681 14924 14952 15110 15252 15371 15474 15664 21005 21302 21600 21635 21706 21755 22098 22240 22314 22355 22459 22716 23844 23940 25225 26132 28953 29015 29116 29737 30196 30258 30607 30686 31502 32197 32549 33228 33993 34267 35397 35629 36020 37042 37244 37354 37769 38003 38078 38080 38153 38481 39249 39347 39645 39943 39995 40107 40380 40680 41079 41229 41442 41543 41729 41914 43204 43297 45132 45585 45689 46779 48058https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/691/A249?format=asciidefaultJ/A+A/691/A249/sourcesList of studied sourcesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaiaIDGaia name identification, Gaia NNaaameta.id;meta.maincharNameOther namemeta.idcharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainSimbadSimbad column added by the CDSmeta.ref.urlcharJ/A+A/691/A249/table1Individual Gaia alerts eclipse (or brightness minima) epochs for DNe systemsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGaiaIDGaia name identification, Gaia NNaaameta.id;meta.maincharNNumber of detected eclipsesmeta.numberfloatETotal number of eclipse observationsmeta.numberfloatHJDHeliocentric Julian Date minus 2450000dtime.epochdouble